We investigate the evolution of isolated , zero and finite temperature , massive , uniformly rotating and highly magnetized white dwarf stars under angular momentum loss driven by magnetic dipole braking .
We consider the structure and thermal evolution of white dwarf isothermal cores taking also into account the nuclear burning and neutrino emission processes .
We estimate the white dwarf lifetime before it reaches the condition either for a type Ia supernova explosion or for the gravitational collapse to a neutron star .
We study white dwarfs with surface magnetic fields from 10 ^ { 6 } to 10 ^ { 9 } G and masses from 1.39 to 1.46 ~ { } M _ { \odot } and analyze the behavior of the white dwarf parameters such as moment of inertia , angular momentum , central temperature and magnetic field intensity as a function of lifetime .
The magnetic field is involved only to slow down white dwarfs , without affecting their equation of state and structure .
In addition , we compute the characteristic time of nuclear reactions and dynamical time scale .
The astrophysical consequences of the results are discussed .